Can galactic magnetic fields diffuse into the voids?
Oindrila Ghosh, Axel Brandenburg, Chiara Caprini, Andrii Neronov, Franco Vazza
TL;DR
The paper argues that cosmic voids are not vacuum but conducting plasmas, which makes diffusion of magnetic fields from galaxies extremely inefficient. Through analytical considerations and mean-field MHD simulations, it shows that even with turbulent diffusion, the outward spread of dynamo-generated galactic fields into voids remains limited to sub-Mpc scales within a Hubble time, and quadrupolar configurations decay as $\sim r^{-2}$ inside the diffusion radius, forming a magnetized magnetosphere around galaxies. Consequently, filling the vast volumes of voids with magnetization by astrophysical processes alone is implausible, favoring primordial magnetogenesis as the natural explanation for space-filling weak void fields. The work also outlines observational signatures via Faraday rotation measures, indicating current data are close to, but generally below, detection thresholds, while future probes (e.g., FRB RM studies) could help discriminate between primordial and astrophysical origins.
Abstract
Cosmic voids are magnetized at the level of at least $10^{-17}$ G on Mpc scales, as implied by blazar observations. We show that an electrically conducting plasma is present in the voids, and that, because of the plasma, \emph{diffusion} into the voids of galactic fields generated by a mean-field dynamo is far too slow to explain the present-day void magnetization. Indeed, we show that even in the presence of turbulence in the voids, dynamo-generated galactic fields diffuse out to a galactocentric radius of only 200-400 kpc. Therefore, it is challenging to meet the required volume filling-factor of the void magnetic field. We conclude that a primordial origin remains the most natural explanation to the space-filling weak fields in voids.
